15. Structure and Dynamics of a Polar Crown Cavity as Observed by SDO/AIA

Introduction

Cavities have been observed above the solar limb for a long time using white-light coronographs (e. g., [1]). However, study of their structure and dynamical behaviour has only become possible recently with observation from space-based missions such as SoHO, TRACE, STEREO, Hinode and SDO. Here, we use the capabilities of SDO/AIA ([2], [3]) to determine the structure and evolution of a polar crown filament within a cavity over a period of 12 hours. The high time cadence, spatial resolution and temperature coverage provide a consistent picture of the filament material and the dynamics of the structure.

Structure of the Polar Crown Cavity

The cavity was observed on 13 June 2010 in several SDO/AIA channels providing a temperature coverage of the structure from 50000 K to several million degrees. The cavity is characterised by

Cool and hot plasma off the limb located at the bottom of the cavity (Fig. 1a and 1b)

A dark cavity (egg-shape structure) seen as concentric ellipses (Fig. 1b-d). The edges of the cavity are clearly seen in the hotter channels (Fig. 1c and 1d)

Elongated barbs seen as dark material (Fig. 1b-d) connecting the photosphere/chromosphere to the corona, and supplying/evacuating the material to/from the polar-crown filament

As most of the material is located in the dips of the cavity, the stability of the structure corresponds to a magnetohydrostatic equilibrium in which the upward magnetic-field curvature balances the gravitational force.

Eruption of the cavity

After hours of stability, the cavity starts to erupt. The evolution is characterised by two main phases:

A slow rise at a characteristic speed of 0.6 km.s-1

A fast motion corresponding to the acceleration phase with a characteristic speed of 25 km.s-1 at the end of the time series (before the cavity has left the SDO/AIA field-of-view)

The movie below shows the evolution of the cavity in the 171Å channel: (left) from SDO/AIA images, (right) from time slices indicated on the left-hand side images. One can see that a large part of the material within the cavity is falling down to the bottom of the corona and/or the chromosphere during the eruption.

Figure 2: (left) Evolution of the cavity during the eruption, (right) time slices at three different locations.

Conclusions

The observations of the cavity provided by SDO/AIA are a good example of the need for high spatial and time resolutions combined with a broad temperature coverage. The thermal structure of the cavity suggests that a large amount of the material is located at the bottom of the cavity. The plasma is sustained in an equilibrium state by the upward curvature of the magnetic field which counteracts the gravitational force. The cavity is thus a density depletion at the bottom of which plasma from 50000K to at least 1 million degrees sits.

It is important to remember that the observations described above correspond to the projection onto the plane of the sky, and thus do not provide a complete picture of the cavity. In a forthcoming study, we will provide a more complete 3D picture of the cavity and polar crown filament by combining SDO/AIA and STEREO-A/SECCHI/EUVI observations. This aims to investigate how the cavity can be destabilised: by external (i.e. flare, CME) and/or internal (i.e. kink instability, mass loading) triggers.

A detailed description of these observations is given in [4]. The SDO/AIA data have been retrieved from the UCLan SDO archive. We thank NASA/SDO and the SDO/AIA science team.